A Catalog of Spectral Properties for DESI DR1 Quasars

arXiv:2610.31416 · astro-ph.GA · Submitted 2026-10-22 · Read on arXiv

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Introduction to the show: ident: Astrophysics Radio. Generated commentary on the latest astrophysics papers.

Vera: We're looking at the paper: "A Catalog of Spectral Properties for DESI DR1 Quasars".

Jocelyn: Here's the gist of the paper. The gist The Dark Energy Spectroscopic Instrument (DESI) survey provides a value-added catalog of spectral properties for 1,717,774 unique quasars in DESI Data Release 1, enabling studies of quasar demographics and black hole accretion.

Vera: Data Acquisition and Sample Characteristics The DESI DR1 sample comprises 1,717,774 unique quasars with 1,774,723 spectra derived from optical imaging and spectroscopy The targets are selected primarily from optical imaging in g, r, z bands and WISE W1, W2 using a random forest algorithm to improve quasar selection efficiency The main-survey selection achieves high quasar purity at magnitude range 16.5 2.1) DESI deploys 5,000 fiber-positioning robots with ten corresponding spectrographs with three arms: blue (B; 3600−5800 Å), red (R; 5760−7620 Å), and near-infrared (Z; 7520−9824 Å) The combined wavelength coverage is 3600 − 9824 Å with resolution R ∼ 2000 − 5200 (arm-dependent) and a fixed pixel size of 0.8 Å Spectral Fitting Methodology The spectral measurements are performed following the practice in earlier work using the publicly available code PyQSOFit Each quasar spectrum was first corrected for the Milky Way extinction using the dust maps (Schlegel et al.

Jocelyn: 1998; Schlafly & Finkbeiner 2011) and then shifted to the rest frame for spectral analysis For quasars at redshift z < 1.0, host-galaxy decomposition is performed with priors to remove stellar contamination The continuum is modeled with a combination of a power law, a third-order polynomial, and Fe II templates fitted to line-free regions of the spectrum Emission and absorption lines are then modeled with multiple Gaussian components, allowing for measurements of peak wavelength, line fluxes, luminosities, full width at half maximum (FWHM), equivalent widths (EW), and centroid wavelength Derived Physical Quantities Several key physical properties are derived from the spectral fits: Bolometric luminosities are estimated from continuum luminosity at 1350 Å, 3000 Å, and 5100 Å using empirical bolometric corrections BC = 3.81, 5.15, and 9.26, respectively BH masses were estimated from the continuum and broad emission lines using SE virial relations (Vestergaard & Peterson 2006) The fiducial BH mass recipes on Hβ, Mg II and C IV are adopted as in previous work The Eddington ratio is calculated using Lbol/LEdd ≡ Lbol/(1.26×1038 MBH) Systemic redshifts are derived by estimating zsys,line for each line with a > 3σ flux detection and spectral coverage Npix > Npix,max/2 The adopted zsys is the inverse-variance-weighted mean of the remaining lines The catalog includes local fits to several optical coronal lines, including

Ne V: λ3426,

Fe VII: λ5722,

Fe VII: λ6088, and

Fe XI: λ7893 The catalog is intended as a community resource for studies of quasar demographics, black hole accretion, emission-line physics, and the connection between the broad-, coronal-, and narrow-line regions The catalog includes local fits to ten coronal lines These measurements can help connect the BLR, CLR, and NLR to the underlying accretion state Emission-line ratios are tested as a function of L/LEdd across different MBH quintiles to disentangle accretion-rate trends from BH-mass dependence These ratios are sensitive to the ionizing SED in the EUV and soft X-ray regime, which cannot be observed directly for the vast majority of quasars.

Vera: The large sample size and homogeneous measurements provided by this catalog open new opportunities for statistical studies of quasar physics.

Title and authors: Vera: Okay, so the team has put together some improvements they suggest for this catalog, and we need to unpack those changes. They’re focusing on making the redshift determination better.

Jocelyn: They propose improving redshift determination for DESI DR1 quasars by using systemic redshifts zsys instead of pipeline redshifts zpip for low-redshift objects or spectra with very low signal-to-noise SNR less than one.

Subrahmanyan: That makes sense because the authors suggest this mitigates biases from host-galaxy features and/or low SNR template degeneracies that can bias line centroid based systemic redshift recipes.

Vera: Then they enhance black hole mass estimation by adopting a fiducial BH mass recipe based on the redshift. They select one rule: they adopt the Mg II mass for zero point six to two point two when available, otherwise the H beta mass for redshift less than zero point eight or the C IV mass for redshift greater than one point eight.

Jocelyn: That's a specific rule, which is good because it gives us a concrete way to handle those uncertainties when we don't have all the data points available.

Subrahmanyan: I think that’s a smart approach because it tries to balance the different mass estimators based on redshift.

Vera: They also developed a new diagnostic tool using emission-line ratios as a proxy for the accretion state of the central SMBH by analyzing how those ratios vary systematically with Eddington ratio across different line pairs, including optical, UV BEL, and coronal lines.

Jocelyn: That sounds like it moves us beyond just looking at one line ratio and starts looking at how the entire set of emission lines behaves together relative to accretion rate.

Subrahmanyan: That’s a way to probe the physics of the ionizing SED in the EUV and soft X-ray regime, which we can’t observe directly for most quasars.

Vera: They also implemented an improved quasar selection pipeline by integrating machine learning classifiers like QuasarNet and post-processing pipelines for Mg II doublet selection to improve purity in magnitude ranges where DESI DR1 reaches fainter magnitudes.

Jocelyn: So they’re trying to clean up the input sample itself, which is a necessary step before you do all that detailed spectral fitting.

Subrahmanyan: Improving the selection pipeline should lead to a more homogeneous sample, which helps when we try to compare these results with other surveys.

The paper's summary: Vera: So to wrap up on this paper, the main implication is that by providing this catalog of spectral properties for DESI DR1 quasars, we’re getting a much richer dataset for studying black hole accretion and demographics.

Jocelyn: It’s about having these measurements—luminosities, masses, Eddington ratios—all tied together in one place to study the relationship between different AGN components.

Subrahmanyan: From my side, I see this as a foundation for physically motivated modeling of AGN emission. We can use these derived quantities to test our models of how structure forms and how SMBHs grow in those environments.

Vera: And they’ve done a lot to connect the broad line region, the coronal line region, and the narrow-line region through those local fits to coronal lines.

Jocelyn: That connection is key because it lets us track how gas requiring photon energies of approximately one hundred eV or more in the CL gas tracks the NLR with no measurable change in continuum hardness across their range.

Subrahmanyan: That implies that these ratios may serve as a proxy for the accretion state of the central SMBH where we might not have a reliable single-epoch mass and thus L over L Edd available.

Vera: Overall, this catalog is designed to serve as a foundation for a wide range of applications, from precision redshift measurements to physically motivated modeling of AGN emission.

Jocelyn: We see the comparison with SDSS quasar catalogs shows good overall consistency between DESI and SDSS measurements of masses.

Subrahmanyan: But they also found some differences in how the three catalogs compare; for instance, their Mg II-based masses broadly agree, but there are broader tails toward large discrepancies between the two mass estimates than those of DR16Q.

Vera: That comparison with SDSS DR16Q is very telling because it allows us to investigate quasar spectroscopic variability on a statistical basis across both surveys.

Jocelyn: So in summary, the paper "A Catalog of Spectral Properties for DESI DR1 Quasars" provides a large, uniformly characterized sample for studying quasar physics.

Subrahmanyan: It's a resource designed to be a foundation for many applications in AGN research and cosmology.

The paper's improvements: Vera: So we've seen that this catalog is a big data set for quasars, but now they’re suggesting some specific ways to make it even better and more useful.

Jocelyn: Right, like improving how we figure out where these quasars are in the sky or what kind of black holes they host.

Vera: Exactly. They propose using systemic redshifts instead of pipeline ones for low-redshift objects or those with low signal-to-noise data. The idea is that this helps avoid biases from host galaxy features and template degeneracies when we try to estimate the redshift from line centroids.

Subrahmanyan: That’s a practical fix because those line centroid recipes can be really sensitive to weird stuff in the host galaxy, like absorption lines, which messes up the systemic redshift.

Jocelyn: And then they have this specific rule for black hole mass estimation based on redshift. They suggest using Mg II mass if you're between zero point six and two point two, or H beta mass if you're below zero point eight, or C IV mass if your redshift is greater than one point eight.

Vera: It’s a way to adopt a fiducial recipe that changes based on where the quasar is in cosmic time. That gives us more control over the uncertainty in those masses.

Subrahmanyan: I think that’s sensible because it acknowledges that different tracers—Mg II, H beta, C IV—have different dependencies on redshift and whatever physical state the quasar is in at that epoch.

Jocelyn: Then they’ve developed a new way to look at emission-line ratios as a proxy for the black hole's accretion state. They want us to analyze how those ratios vary systematically with Eddington ratio across optical, UV BEL, and coronal lines together.

Vera: That moves us beyond just looking at one line ratio and starts looking at the whole set of emission lines together to gauge the accretion rate. That should be a much stronger diagnostic tool for what's happening around the black hole.

Subrahmanyan: It’s a way to probe that ionizing SED in the EUV and soft X-ray regime that we can't see directly, which is super valuable for understanding the physics of accretion itself.

Jocelyn: They also improved the input sample by integrating machine learning classifiers like QuasarNet and post-processing for Mg II doublet selection. This makes the initial sample much cleaner, especially at fainter magnitudes where DESI DR1 gets to.

Vera: So they’re trying to get a more homogeneous sample before you do all that detailed spectral fitting on the emission lines. That should really improve the reliability of our final catalog products.

Subrahmanyan: It makes sense; better input data leads to better physics tests in the end. This whole effort is building a foundation for those larger statistical studies we need for quasar evolution and demographics.

Vera: These improvements, though, they also highlight some things that are still tricky—like the discrepancies between different mass estimates or how much variability we can really pin down across both surveys.

Jocelyn: That’s what I want to dig into next—how those differences between DESI and SDSS quasars actually look when you put them together for time-domain studies.

Conclusion: Vera: So we’ve looked at the specific improvements they made to this catalog of spectral properties for DESI DR1 quasars, focusing on better redshift estimates and more robust black hole mass calculations.

Jocelyn: Right, they're essentially tuning the instruments and the recipes so that when we look at these quasars, we get cleaner numbers for where they are in space and how big their central engines actually are.

Subrahmanyan: And from a theoretical standpoint, having these refined measurements for L bol and lets us test our models of structure formation much more directly.

Vera: The main implication is that this catalog provides a much more reliable foundation for studying quasar demographics and accretion physics because the input data is cleaner and the derived quantities have fewer systematic errors.

Jocelyn: It means we can start doing those long-timescale studies of variability you mentioned earlier with a higher confidence level because we’re not fighting as much noise in our redshift or mass measurements.

Subrahmanyan: If these improved masses and accretion ratios hold up across the sample, it gives us a better handle on how black hole growth relates to the properties of the host galaxy environment at different cosmic epochs.

Vera: It’s a solid resource for anyone studying emission-line physics and connecting the broad, coronal, and narrow line regions because those local fits to coronal lines are now more reliable.

Jocelyn: I think what they’ve done is give us a really strong tool to link different parts of the AGN structure together based on these new ratios.

Subrahmanyan: If we can use those ratios as a proxy for the accretion state, that opens up a whole new avenue for understanding how different fueling mechanisms drive quasars.

Vera: So, to recap this paper, "A Catalog of Spectral Properties for DESI DR1 Quasars," they’ve sharpened the tools and made the data cleaner.

Jocelyn: It’s a big step forward for using DESI data in time-domain studies because the characterization is now much more consistent.

Subrahmanyan: We need to see if these improved measurements hold up when we look at larger samples across different redshift bins to confirm their cosmological relevance.

Vera: That’s what we'll be watching next, as they move toward those statistical comparisons between DESI and SDSS quasar catalogs.

Jocelyn: We’ll keep an eye on that comparison for any weird systematic shifts in the mass measurements across the whole field.

Qiaoya Wu, Yue Shen

Department of Astronomy, University of Illinois at Urbana-Champaign · National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign

astro-ph.GA

Submitted: 2026-10-22

Updated: 2026-10-22

Comments: 17 pages, 10 figures, and 2 tables. Preprint version; comments and feedback are welcome

Code: https://github.com/QiaoyaWu/desi-dr1-quasar-vac

License: http://creativecommons.org/licenses/by/4.0/

The gist: The gist The Dark Energy Spectroscopic Instrument (DESI) survey provides a value-added catalog of spectral properties for 1,717,774 unique quasars in DESI Data Release 1, enabling studies of quasar

Key concepts

Bolometric Luminosity Estimation: This is an estimate of the total energy output from a quasar by measuring its continuum luminosity at specific wavelengths (like 1350 Å, 3000 Å, and 5100 Å) and applying empirical conversion factors. This helps determine the quasar's total energy output across all wavelengths.
Black Hole Mass Estimation: Black hole masses are calculated using virial relations that relate the width of broad emission lines to the mass of the central black hole. Different recipes are used depending on the redshift, prioritizing Mg II for certain redshift ranges to ensure consistency and accuracy.
Coronal Line Diagnostics: The catalog includes local fits to high-ionization coronal lines like [Ne V] and [Fe VII]. These lines originate from the hot gas surrounding the black hole. Analyzing their ratios helps connect the broad-line region, coronal line region, and narrow-line region to understand the central accretion state.

Summary

The gist The Dark Energy Spectroscopic Instrument (DESI) survey provides a value-added catalog of spectral properties for 1,717,774 unique quasars in DESI Data Release 1, enabling studies of quasar demographics and black hole accretion.

Data Acquisition and Sample Characteristics

The DESI DR1 sample comprises 1,717,774 unique quasars with 1,774,723 spectra derived from optical imaging and spectroscopy The targets are selected primarily from optical imaging in g, r, z bands and WISE W1, W2 using a random forest algorithm to improve quasar selection efficiency The main-survey selection achieves high quasar purity at magnitude range 16.5 2.1) DESI deploys 5,000 fiber-positioning robots with ten corresponding spectrographs with three arms: blue (B; 3600−5800 Å), red (R; 5760−7620 Å), and near-infrared (Z; 7520−9824 Å) The combined wavelength coverage is 3600 − 9824 Å with resolution R ∼ 2000 − 5200 (arm-dependent) and a fixed pixel size of 0.8 Å

Spectral Fitting Methodology

The spectral measurements are performed following the practice in earlier work using the publicly available code PyQSOFit Each quasar spectrum was first corrected for the Milky Way extinction using the dust maps (Schlegel et al. 1998; Schlafly & Finkbeiner 2011) and then shifted to the rest frame for spectral analysis For quasars at redshift z < 1.0, host-galaxy decomposition is performed with priors to remove stellar contamination The continuum is modeled with a combination of a power law, a third-order polynomial, and Fe II templates fitted to line-free regions of the spectrum Emission and absorption lines are then modeled with multiple Gaussian components, allowing for measurements of peak wavelength, line fluxes, luminosities, full width at half maximum (FWHM), equivalent widths (EW), and centroid wavelength

Derived Physical Quantities

Several key physical properties are derived from the spectral fits:

** Bolometric luminosities are estimated from continuum luminosity at 1350 Å, 3000 Å, and 5100 Å using empirical bolometric corrections BC = 3.81, 5.15, and 9.26, respectively BH masses were estimated from the continuum and broad emission lines using SE virial relations (Vestergaard & Peterson 2006) The fiducial BH mass recipes on Hβ, Mg II and C IV are adopted as in previous work The Eddington ratio is calculated using Lbol/LEdd ≡ Lbol/(1.26×1038 MBH) Systemic redshifts are derived by estimating zsys,line for each line with a > 3σ flux detection and spectral coverage Npix > Npix,max/2 The adopted zsys is the inverse-variance-weighted mean of the remaining lines The catalog includes local fits to several optical coronal lines, including [Ne V] λ3426, [Fe VII] λ5722, [Fe VII] λ6088, and [Fe XI] λ7893 The catalog is intended as a community resource for studies of quasar demographics, black hole accretion, emission-line physics, and the connection between the broad-, coronal-, and narrow-line regions The catalog includes local fits to ten coronal lines These measurements can help connect the BLR, CLR, and NLR to the underlying accretion state Emission-line ratios are tested as a function of L/LEdd across different MBH quintiles to disentangle accretion-rate trends from BH-mass dependence These ratios are sensitive to the ionizing SED in the EUV and soft X-ray regime, which cannot be observed directly for the vast majority of quasars. The large sample size and homogeneous measurements provided by this catalog open new opportunities for statistical studies of quasar physics. The substantial overlap with previous spectroscopic surveys and synergy with ongoing and future time-domain and photometric programs make this dataset a valuable resource for studies of quasar variability and evolution. The multi-year baseline between SDSS and DESI is well-suited for identifying such long-timescale spectral variability. The catalog is designed to serve as a foundation for a wide range of applications, from precision redshift measurements to physically motivated modeling of AGN emission. The catalog includes local fits to coronal emission lines in DESI DR1 quasar spectra These high ionization potentials make them powerful diagnostics of the EUV/softX-ray continuum. Ratios involving [Ne V] and lowerionization lines can also improve AGN identification at redshifts where standard optical diagnostics are inaccessible. The ratios between the CLs and the narrow Balmer lines are also flat, indicating that the CL gas requiring photon energies of ≈100 eV or more tracks the NLR with no measurable change in the soft X-ray/EUV continuum hardness relative to the optical lines across our range. These additional line ratios may serve as a proxy for the accretion state of the central SMBH where a reliable single-epoch mass, and hence L/LEdd, is unavailable. The comparison with SDSS quasar catalogs demonstrates overall consistency The DESI masses broadly agree with those measured from SDSS spectra Overall, the Mg II-based masses are consistent with those derived from Hβ and C IV Some differences among the three catalogs are expected from the spectral-fitting methodology. The DESI DR1 distributions also show broader tails toward large discrepancies between the two mass estimates than those of DR16Q. The substantial overlap between the SDSS and DESI DR1 quasar samples provides a valuable opportunity to investigate quasar spectroscopic variability on a statistical basis. By presenting spectral measurements from both surveys within a consistent analysis framework, our data products enable systematic time-domain studies of quasars across a large, uniformly characterized sample. The catalog is designed to serve as a foundation for a wide range of applications, from precision redshift measurements to physically motivated modeling of AGN emission. All products from this work, including the catalog, input fitting parameters, individual FITS outputs, Python notebooks, and update notes can be accessed from our data server and GitHub repository. The comparison of redshift and virial BH mass measurements between DESI DR1 quasars and their SDSS DR16Q counterparts shows good overall consistency between the DESI and SDSS measurements The middle and right panels compare the MBH measurements.

Improvements for AI systems

Improved redshift determination for DESI DR1 quasars by using systemic redshifts (zsys) instead of pipeline redshifts (zpip) for low-redshift objects or spectra with very low signal-to-noise (SNR less than 1). This mitigates biases from host-galaxy features and/or low-SNR template degeneracies that can bias line-centroid based systemic redshift recipes.
Enhanced black hole mass estimation by adopting a fiducial BH mass recipe based on the redshift, which is selected according to a specific rule: we adopt the Mg II mass for 0.6 ≤ zpip ≤ 2.2 when available, otherwise the Hβ mass for zpip ≤ 0.8 or the C IV mass for zpip ≥ 1.8.
Development of a new diagnostic tool using emission-line ratios as a proxy for the accretion state of the central SMBH, specifically by analyzing how emission-line ratios vary systematically with Eddington ratio across different line pairs (optical, UV BEL, and coronal lines).
Implementation of an improved quasar selection pipeline by integrating machine learning classifiers like QuasarNet and post-processing pipelines for Mg II doublet selection to improve quasar purity in magnitude ranges where DESI DR1 reaches fainter magnitudes.
Creation of a comprehensive value-added catalog that includes local fits to coronal lines such as [Ne V] lambda 3426, [Fe VII] lambda 5722, and [Fe VII] lambda 6088, allowing for studies connecting the broad-, coronal-, and narrow-line regions.
Statistical comparison of DESI DR1 quasar measurements with SDSS DR16Q counterparts to quantify systematic differences in redshift estimates and black hole mass calculations, particularly identifying sources where C IV -based masses are much lower than their Mg II-based masses.

Abstract

The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year spectroscopic survey designed to map the large-scale structure of the Universe and obtain spectra for millions of galaxies and quasars over a wide redshift range. We present a value-added catalog of spectral properties for 1,717,774 unique quasars (1,774,723 spectra) in the DESI Data Release 1. We perform a uniform spectral decomposition of the quasar continuum, host galaxy emission (at z<1), and emission, and measure the line properties of major broad and narrow emission lines from Ly α to H α covered by DESI spectra. We also provide single-epoch black hole mass estimates (from H β,, and), bolometric luminosities, and Eddington ratios for these quasars. We provide systemic redshifts that account for the intrinsic velocity shifts of individual lines; they agree with the DESI pipeline redshifts to within 500 km s-1 for 88.6% of the sample, and are most useful at z>1 where the pipeline redshift is heavily constrained by blueshifted high-ionization lines. We also provide local fits to several optical coronal lines, including lambda3426, [7] lambda5722, [7] lambda6088, and [11] lambda7893. We show that several emission-line ratios, including those involving coronal lines, vary systematically with Eddington ratio. The catalog is intended as a community resource for studies of quasar demographics, black hole accretion, emission-line physics, and the connection between the broad-, coronal-, and narrow-line regions.